The Role of Carbon in Interstellar Extinction CYC3SUPPLEMENTAL

Details The Role of Carbon in Interstellar Extinction CYC3SUPPLEMENTAL The Role of Carbon in Interstellar Extinction CYC3SUPPLEMENTAL

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4327s&link_type=abstract

HST Proposal ID #4327

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Hst Proposal Id #4327

Scientific paper

We propose to measure carbon depletions in two stars representing extremes in UV extinction behavior, in order to constrain models for interstellar dust which attribute the extinction to carbon in various forms. While a larger sample eventually will be needed, even the small dataset we propose to acquire here will be sufficient to provide some very significant results: (1) we will determine whether the 2175A bump or the far-UV rise (or both) are due to carbon; (2) if so, we will determine whether the same form of carbon can be responsible for both features. The high total extinctions of our target stars will provide greater leverage for discriminating among the models than in for other HST studies. Most of the observing time will be dedicated to measuring the weak C II] line at 2325A with sufficient sensitivity to detect it for carbon depletions up to a factor of 3 (which is greater than any carbon depletion sug- gested by previous observations); we will also observe the strong C II line at 1334A, in order to measure damping wings and help ascertain the column density (and refine the f-value for the 2325A line); and we will observe C I and CO. We will also include the H I 1216A line in our observations, and we will use indirect indicators of the H2 column density in order to estimate absolute depletions.

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